Non-Sobolev modelling of radiation-pressure-driven flows in active galactic nuclei

被引:12
作者
Chelouche, D [1 ]
Netzer, H
机构
[1] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel
[2] Tel Aviv Univ, Wise Observ, Raymond & Beverly Sackler Fac Exact Sci, IL-69978 Tel Aviv, Israel
关键词
radiative transfer; methods : numerical; ISM : jets and outflows; galaxies : active; galaxies : nuclei; quasars : absorption lines;
D O I
10.1046/j.1365-8711.2003.06840.x
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present a new general scheme for calculating the structure and dynamics of radiation-pressure-driven photoionized flows. The new method goes one step beyond the Sobolev approximation. It involves a numerical solution of the radiative transfer in absorption lines, including the effects of differential expansion and line interactions such as line locking and blanketing. We also present a new scheme for calculating the radiation pressure due to trapped line photons in finite, differentially expanding flows. We compare our results for the radiation pressure force with those obtained using the Sobolev approximation and show the limitations of the latter. In particular, we demonstrate that the Sobolev method gives a poor approximation near discontinuity surfaces and its neglect of line blanketing can lead to erroneous results in high-velocity flows. We combine the newly calculated radiation pressure force with self-consistent photoionization and thermal calculations to study the dynamics and spectral features of broad absorption-line flows and highly ionized gas flows in active galactic nuclei (AGN). A comparison with Sobolev-type calculations shows that the latter overestimates the terminal velocity of the flow and, conversely, underestimates its opacity. We also show that line locking on broad emission lines can have a significant effect on the dynamics and spectral features of AGN flows.
引用
收藏
页码:223 / 232
页数:10
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